The compact radio source components in our e-MERLIN images account for almost all of the integrated radio emission in our targets.
Even the faintest components that we measure from our images have L-band flux densities \(> 0.3\)  mJy (Table REF ),
which, at their redshifts,
imply L\(_{\rm 1.4}\)  \(>5\times 10^{24}\)  W Hz\(^{-1}\) , or SFRs greater than a few 1000 M\(_{\odot }\)  yr\(^{-1}\) , taking
well-used calibrations between SFR and L\(_{\rm 1.4}\)  [1]}, [2]}. Estimates of the SFR from integrated L\(_{\rm 1.4}\)  can be
much higher. These derived SFRs are 1-2 orders of magnitude larger than the SFRs of typical QSOs at \(z\sim 1\) 
[3]}, [4]}, [5]}.
Quite simply, the radio luminosities of our sample are too large for star-formation to be an important contributor to the emission we
detect with FIRST or e-MERLIN. Even among co-eval `radio-quiet' QSOs, with L\(_{\rm 1.4}\)  fainter than our targets by an order
of magnitude, star-formation is not found to dominate the integrated 1.4 GHz radio emission [6]}.
Therefore, we can confidently continue with the notion that the radio differences we see are due to AGN-powered processes.
